FMOS and UKIDSS Galactic Astronomy

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FMOS and UKIDSS Galactic Astronomy

• Phil Lucas UHerts

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Outline

• 1) UKIDSS galactic surveys and FMOS
• 2) Brown Dwarf Science with FMOS
• 3) X-ray sources and FMOS
• 4) Mapping nebulae with FMOS

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UKIDSS The UK Infrared Deep Sky Survey

• WFCAM
• 0.8-2.5mm imager FOV 0.76 deg2/tile Forward
  mounted Cass focus on UKIRT
• UKIDSS
• UKESOJapan 5 surveys from 2004
  UDS 0.76 deg2 DXS
  35 deg2 GPS 1800 deg2
  GCS gt1000 deg2 LAS
  4000 deg2

- Galactic Plane at blt5 degrees.
- Galactic Clusters, eg. Orion, Pleiades. -
High latitude survey.
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Brown Dwarfs background
M6
L5
T8
Brown dwarfs spectral types are a cooling
sequence. The spectral types have been determined
using 2MASS and SLOAN sources, eg.Kirkpatrick et
al.(1999, ApJ 519,802) They range from near M6
soon after formation to T8 and later, not yet
discovered types at ages several Gyr. THE GCS and
GPS will mostly see young M and L type brown
dwarfs.
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Brown dwarfs, UKIDSS and FMOS (1)

• The UKIDSS science goals are to measure the IMF
  in a range of different environments and study
  brown dwarf formation and kinematics.
• The GCS will survey 10 nearby clusters at JHK to
  K18.4. The younger clusters have high source
  densities -gt FMOS targets.
• The GPS will survey half the galactic plane at
  JHK to K19. Hundreds of clusters will be
  detected but most will be quite distant and
  crowded. FMOS will be invaluable for testing
  cluster membership.
• SIRTF, ASTRO-F and MSX surveys.

Perseus OB2 Taurus-Auriga Orion
Scorpio-Centaurus Alpha-Per Pleiades
Hyades Praesepe
Coma-Ber IC4665
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Brown Dwarfs, UKIDSS and FMOS (2)
Credit 2MASSAll Sky Survey
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Brown Dwarfs, UKIDSS and FMOS (3)

• What will FMOS spectra tell us?
• - confirm cluster membership reliable LF.
• - 0.9 1.8 um spectra yield Effective
  Temperature, spectral type and surface
  gravity.
• - This allows determination of location on
  HR diagram, yielding age corrected IMF and the
  star formation history of the cluster.
• - Effects of circumstellar matter on
  spectra, eg. scattered light, and externally
  excited SIII and accretion powered Hydrogen
  recombination lines will be measured with a large
  sample (Paschen series).
• FMOS spare fibres will be vital for good
  background subraction.

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Brown Dwarfs, UKIDSS and FMOS (4)
(Lucas et al.2001, MNRAS 326,695)
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Chandra / UKIDSS sources and FMOS

• The UKIDSS Galactic Plane Survey will identify IR
  counterparts to thousands of Chandra and XMM
  X-ray sources.
• Chandra Galactic Centre study. CVs, Neutron
  star/White Dwarf binaries, wind accreting
  binaries, active stars? Background AGN?
• High source density in the plane typically 2
  sources per Chandra error circle (0.3 to 1
  arcsec). FMOS will be needed for a large study to
  understand the various populations.
• FMOS science (1) detect accretion signatures
  HI lines
• (2) detect and identify
  faint stellar companion.

CHANDRA - ACIS image
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Chandra sources and FMOS (2)

• The Chandra Deep Field.
• Other UKIDSS GPS fields.
• Nearby spiral galaxies.
• In all these cases IR spectroscopy is desired
  to identify X-ray sources.

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High Mass Star Formation Regions
HST/WFPC1 image of a star forming region

• Star formation regions containing O-type stars
  often have pervasive nebulosity with a wide range
  of excitation conditions. Analysis of this such
  regions is important to understand the effect of
  environment on star and brown dwarf formation and
  the IMF.
• FMOS can sample nebular emission lines in 400
  places.
• Useful lines in the ZJH bands are SIII at 953
  nm, HeI at 1080 nm, and the Paschen series of
  hydrogen.

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SNe remnants, microquasars and PNe
Rudy et al.(2001, ApJ 121, 362) spectra of a PN

• FMOS can provide information on the excitation
  conditions in all types of high excitation
  nebulae. MOIRCS will be more useful for low
  excitation nebulae. The UKIDSS GPS will identify
  the infrared targets for which multi-fibre data
  will be useful.
• Multi-epoch FMOS data over a period of a few
  years will help us to understand the changing
  excitation conditions in highly excited and fast
  moving jets and knots, such as those observed in
  the microquasar SS433 or in planetary nebulae
  such as the Helix nebula.

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Conclusions

• FMOS and similar IRMOSes will be essential for
  the exploitation of data from the UKIDSS Galactic
  Plane Survey and Galactic Clusters Survey.
• For Galactic Science optical MOSes are of little
  use. FMOS will benefit but from a synergy of
  X-ray, near IR and mid-IR data.